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The Faint End of the Main Sequence

Greenstein, Jesse L. and Neugebauer, G. and Becklin, E. E. (1970) The Faint End of the Main Sequence. Astrophysical Journal, 161 . pp. 519-531. ISSN 0004-637X. doi:10.1086/150556.

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New infrared observations of the two faintest known, late M dwarfs, Wolf 359 and +4°4048B (=VB 10) provide accurate luminosities and moderately well-determined temperatures (2500° and 2250° K, respectively). The photometric observations are fitted to a blackbody energy distribution on the assumption that line and band blocking affect most of the spectrum below 1 μ; the temperature structure is taken as that of a gray body. The resulting data, together with Johnson's observations for dM4 and dM5 stars, which have been reanalyzed, calibrate the faint end of the main sequence, with results given in a table and a figure. The bolometric corrections are very large and increase steeply to 6 mag, so that the faintest known stars are, in fact, not very faint; Wolf 359 has L = 13 X 10^(-4) L_☉, and VB 10 has L = 5 X 10^(-4) L_☉. A statistical discussion of Luyten's faint red stars of large proper motion gives L = 4 X 10^(-4) L_☉. With a conventional mass-luminosity relation, ℳ ≥ 0.09 ℳ_☉ , for stars of known luminosity. Stars of still lower mass, such as L726-8, are difficult to interpret.

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Additional Information:© 1970 The University of Chicago. Received 1970 January 19; revised 1970 February 16. The experimental work was supported by a National Aeronautics and Space Administration grant NGL 05-022-007; the analysis was largely carried out by one of us (J. L. G.) while at the Institute for Advanced Study, and later under AFOSR grant 69-1401.
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NASANGL 05-022-007
Air Force Office of Scientific Research (AFOSR)69-1401
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Official Citation:The Faint End of the Main Sequence Greenstein, J. L., Neugebauer, G., & Becklin, E. E. Astrophysical Journal, vol. 161, p.519-531
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74718
Deposited By: Ruth Sustaita
Deposited On:03 Mar 2017 23:05
Last Modified:11 Nov 2021 05:29

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